It is assumed that the binary pair consists of a smaller minor asteroid in orbit about a larger main asteroid, which encounters a planetary body.
The other is an optimal, single-impulse transfer during encounter to ensure transfer through the ZVC bottleneck and capture of the minor asteroid by the planetary body.
This provides insight into the motion of the minor asteroid about the main asteroid, allowing strategies to engineer the capture process to be developed.
Two capture strategies are then proposed to engineer and extend the possibility for capture of the minor asteroid in binary pair.
In order to develop an engineering model of the problem, first we neglect the mass of the smaller minor asteroid in the binary pair and approximate the model as planar parabolic restricted three-body problem (PPRTBP).
We looked also at other Newtonian (solar quadrupole mass moment, ring of the minor asteroids, Ceres, Pallas, Vesta, Trans-Neptunian Objects) and post-Newtonian (gravitoelectric Schwarzschild solar field) dynamical effects on the Earth Mercury range.
Their nominal peak-to-peak amplitudes are as large as 4 × 105 m (Schwarzschild), 3 × 102 m (Sun's quadrupole), 8 × 101 m (Ceres, Pallas, Vesta), 4 m (ring of minor asteroids), 8 × 10−1 m (Trans-Neptunian Objects).
A 1934 Talk item noted that a "minor planet" — probably an asteroid — had recently been named Vassar, "after the young ladies' seminary of that name".
For the past 10 years, Albert was the only remaining named and numbered asteroid (also called a minor planet) that scientists had lost track of.
A minor planet is the same as an asteroid.
